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RIMAE SIRSALIS Nieves del Río, José Castillo, Eduardo Adarve, Jorge Arranz y Alberto Martos del Grupo de Estudios Lunares “Enrique Silva”. [Página dejada intencionadamente en blanco] - 2 - INTRODUCCIÓN Rimae Sirsalis es un sistema de grietas que comprende dos estructuras de esta clase, Rima Sirsalis y Rima Sirsalis I, siendo la primera mucho más larga y mucho más perceptible que la segunda. Pertenecen a la clase de grietas rectas, cuyo aspecto es diferente del aspecto de las grietas circulares que bordean las cuencas de las grandes estructuras de impacto. Lo que tiene de particular este sistema, para que haya merecido figurar como objetivo 1 en el apartado “Call for Observations 2”, del boletín TLO 3 de ALPO 4, son sus dos características principales: siendo Rima Sirsalis la grieta más larga existente en la cara cislunar (la visible), está situada en una región cuyo suelo es geológicamente distinto de la naturaleza de suelos por los que discurren en general las grietas lunares. En efecto, las grietas lunares (llamadas en latín rimae ) son siempre estructuras volcánicas, generalmente túneles de lava cuyo techo se ha desplomado, o surcos por los cuales fluyó la lava en su día, en favor de la pendiente del suelo. Por esta razón, se las encuentra siempre sobre terrenos magmáticos, como los maria (plural de mare ), los sini (plural de sinus ), los laci (plural de lacus ), o los paludes (plural de palus ), o sea sobre los “mares”, las “bahías”, los “lagos” o las “marismas” lunares. Como ejemplos de esta condición se puede citar a Rimae Hypatia, situada en el Mare Tranquillitatis, a Rima Oppolzer, en Sinus Medii, a Rimae Bürg y Rimae Daniell, en Lacus Mortis y Lacus Somniorum, respectivamente y Rima Hesiodus en Palus Epidemiarum. Pero el sistema Rimae Sirsalis no se encuentra asentado sobre alguna zona de esa clase, sino sobre las terrae , o “tierras altas”, que constituyen los suelos más antiguos (4,5 millares de millones de años) de la superficie lunar, cuya formación es muy anterior a la de los episodios volcánicos (entre 3,8 y 3,2 millares de millones de años) que rellenaron de lava las cuencas de impacto, que se habían formado durante la debatida “época cataclísmica” del Sistema Solar. Por tanto, no parece probable que su origen pueda ser volcánico. La alternativa es que el origen de Rimae Sirsalis sea tectónico. Ahora bien, siendo la Luna un astro geológicamente “casi” muerto y carente de placas tectónicas (mejor dicho, constituyendo toda la superficie lunar una única placa tectónica), no puede atribuirse su origen a movimientos tectónicos horizontales. En la Luna, los únicos movimientos tectónicos de naturaleza endógena posibles, son los verticales, producidos por isostasia (equilibrio de presiones) debida al enfriamiento del astro. Estos movimientos, detectados recientemente por la cámara del satélite LRO 5, han originado fallas de encabalgamiento (thrust faults) sobre terrenos situados en latitudes boreales altas (>60º N) de la superficie lunar 6. Pero estas estructuras tectónicas de origen endógeno no afectan a la latitud media (15º S) de las Rimae Sirsalis, ni han producido estructuras geológicas morfológicamente similares a ellas. 1 Focus On 2 “Propuesta de observación” 3 The Lunar Observer. 4 Association of Lunar and Planetary Observers 5 Lunar Reconnaissance Orbiter. 6 http://lunarnetworks.blogspot.com.es/2010/08/incredible-shrinking-moon.html - 3 - Queda por considerar la posibilidad de que su origen sea tectónico de naturaleza exógena, es decir que fuera una estructura de impacto de segundo orden. En este caso Rimae Sirsalis constituiría una fosa tectónica producida como resultado de un impacto próximo, capaz de desarrollar la energía necesaria para excavar una gran estructura circular, como una cuenca o un gran circo. Bajo esa inmensa cantidad de energía mecánica 7, la onda de choque que sacudiera el suelo lunar circundante, bien podría haber provocado una resquebrajadura del tamaño de la grieta que nos ocupa. La observación telescópica de la Luna ofrece algunos ejemplos elocuentes, quizá bien conocidos del lector, de fallas tectónicas originadas como subproducto de la excavación de una gran estructura de impacto. Como ejemplos de esta condición se puede citar a la grieta más conocida, Vallis Alpina, una fosa tectónica de 180 Km de longitud por 3000 m de anchura, que surgió tras la monstruosa explosión que excavó la cuenca del Mare Imbrium. También son tectónicas Rima Ariadaeus y Rima Hyginus, situadas entre el Mare Vaporum y Sinus Medii. La característica geológica que nos autoriza a adjudicar el origen de una estructura tectónica longitudinal a la formación de otra circular, es su posición radial con respecto a ella: en efecto, tanto Vallis Alpina, como Rima Ariadaeus y Rima Hyginus, apuntan ortográficamente (siguiendo un círculo máximo) al centro de la cuenca del Mare Imbrium. ¿Puede ser Rimae Sirsalis una fosa tectónica bifurcada? Para dar una respuesta afirmativa tendríamos que identificar previamente la gran estructura de impacto capaz de haberla producido. Para ello, empezaremos por visualizar la zona por la que se extienden ambas grietas en la foto 1, en la que se ve que hay dos cuencas de impacto candidatas, la del Oceanus Procellarum y la del Mare Orientale (invisible en la foto). Como puede deducirse al mirar la foto, se trata de una región muy occidental de la cara visible, cuya visibilidad al telescopio está siempre afectada por la oblicuidad de la posición, razón por la cual se debe aprovechar las condiciones de libración en longitud negativa, tanto para la observación visual, como para la fotografía. En la foto 1, tomada el 15 de Marzo de 2014, la libración en longitud 8 era sólo ligeramente favorable, -3º. En la foto 2, tomada el mismo día interponiendo una lente Barlow x2, se identifica las principales estructuras de impacto que salpican la zona de interés, así como una estructura volcánica, Lacus Aestatis. Esta fotografía ilustra la dificultad de asignar origen volcánico al sistema de Rimae Sirsalis, por cuanto la gran mayoría de las estructuras visibles en la zona son de impacto (tectónicas exógenas) y solamente el lacus es de origen volcánico. Aunque el Mare Orientale no es visible desde la Tierra, es fácil comprobar que Rima Sirsalis (la más larga del sistema), al menos en su último tramo, no guarda una posición radial con respecto a esa cuenca, sino que es más bien tangencial a ella. Esta comprobación se puede efectuar mediante cualquier buen programa lunar, como el Atlas Virtual de la Luna (AVL), en cuyo caso conviene seleccionar la pestaña del “Globo Entero” para poder situar el Mare Orientale en el centro de la pantalla. De este modo se podrá comprobar que Rima Darwin, que cruza el circo del mismo nombre y a Rima Sirsalis al Este de dicha estructura de impacto, está mejor situada para este asunto. En suma, el impacto del Mare Orientale no pudo haber originado Rimae Sirsalis. 7 Para ampliar información sobre esta materia, puede consultarse el artículo “Mecánica de Impacto”, A. Martos, Neomenia núm. 45, 9/13. 8 Al final del texto hemos incluido una tabla con los datos de todas las fotografías incluidas en este artículo, así como del instrumental utilizado para obtener cada una. - 4 - Foto 1.- Situación del sistema Rimae Sirsalis en el globo lunar. Nuestra atención se vuelve ahora hacia el Oceanus Procellarum, en busca de la estructura de impacto posible causante de la supuesta grieta tectónica. Un examen detallado de esta región, expuesta en las fotos 3 y 4, cuya calidad deterioraron las condiciones atmosféricas del momento de su captura, revela que Rima Sirsalis (la grieta más larga) arranca del pequeño cráter Sirsalis K (7 Km) y corre en dirección a su hermano algo mayor, Sirsalis J (12 Km). Debido a la consabida oblicuidad de la visión en esta zona y a que en la ocasión de esta fotografía la libración en longitud era muy poco favorable (0º 48’ O), esta trayectoria puede no antojársenos radial con respecto al Oceanus Procellarum. Pero si recurrimos al mapa del programa AVL, entonces ya no nos cabrá duda de que su posición es radial. ¿Hemos dado con la clave? Aunque durante mucho tiempo se ha creído así, por desgracia (¿o por suerte para los investigadores?), últimamente se ha recibido “ novissima argumenta ” que han venido a demostrar que tampoco esta suposición se sostiene. - 5 - Foto 2.- Estructuras de impacto y volcánicas en la zona de Rimae Sirsalis. - 6 - En efecto, los resultados que ha aportado el Proyecto GRAIL 9 (Gravity Recovery And Interior Laboratory) de NASA, descartan que el Oceanus Procellarum se haya originado como cuenca de impacto. El informe de su Investigadora Principal, Maria Zuber, hace añicos la idea de que esta estructura sea una cuenca de impacto rellena de lava por el mecanismo que ha rellenado las restantes, sino que el origen de este magma se atribuye a un penacho de lava procedente del manto interno, ¡exactamente igual que en las erupciones magmáticas que ocurren en las dorsales oceánicas de la Tierra! Ni siquiera existe una cuenca única, pues la forma global de la estructura es poligonal, con ángulos agudos entre las diferentes cavidades, que no han podido ser formados por un impacto colosal, sino por fracturas producidas por las enormes tensiones en la corteza lunar, a que dio lugar el enfriamiento del terreno alrededor del gigantesco penacho de lava ardiente que procedía del interior. En cualquier caso, si el penacho de lava fue originado por un impacto descomunal, hoy no queda rastro del mismo, por lo que la historia del relleno de lava de las cuencas de impacto debe ser re-escrita. Este aldabonazo postrero nos devuelve al punto de partida, ¿qué clase de estructura es Rimae Sirsalis? Afortunadamente, dos investigadores lunares (Lionel Wilson y James Head, británico el primero y norteamericano el segundo) apuntaron otra teoría explicativa de la formación de esta estructura: un dique geológico.
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  • Appendix I Lunar and Martian Nomenclature

    Appendix I Lunar and Martian Nomenclature

    APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei